The Low-Mass End of the IMF in Chamaeleon I

  • Timo Prusti
  • Sacha Hony
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 327)

Abstract

We have compared the low mass and brown dwarf samples of Cha I deduced by optical and infrared techniques. We conclude that optical methods tend to lead to an underestimation of the number of brown dwarfs at least by 15% but possibly by 40 %. Highly complete samples can be constructed by combining optical and mid-infrared samples.

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References

  1. Bontemps, S., André, P., Kaas, A. A., et al. 2001, A&A, 372, 173CrossRefADSGoogle Scholar
  2. López Martí, B., Eislöffel, J., Scholz, A. & Mundt, R. 2004, A&A, 416, 555CrossRefADSGoogle Scholar
  3. Luhman, K. L., Briceño, C., Stauffer, J. R., et al. 2003, ApJ, 590, 348CrossRefADSGoogle Scholar
  4. Persi, P., Marenzi, A. R., Olofsson, G., et al. 2000, A&A, 219,357Google Scholar

Copyright information

© Springer 2005

Authors and Affiliations

  • Timo Prusti
    • 1
  • Sacha Hony
    • 1
  1. 1.ESA/ESTECThe Netherlands

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